Magnetic Reconnection and Associated Transient Phenomena Within the Magnetospheres of Jupiter and Saturn

André, Nicolas; Jackman, C. M.; Kasahara, Satoshi; Kronberg, Elena A.; Vogt, Marissa F.

doi:10.1007/978-1-4939-3395-2_6

Cited by 12 publications

(11 citation statements)

References 145 publications

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“…Recently, Louarn et al . [] also associated radio signatures of reconnection events, occurring in the outer magnetosphere, with energetic particle injections taking place in the inner magnetodisk thus confirming the possible link between reconnection and injection.…”

Section: Introductionmentioning

confidence: 60%

Jupiter's equatorward auroral features: Possible signatures of magnetospheric injections

et al. 2014

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The present study investigates the characteristics of ultraviolet auroral features located equatorward of the main emission appearing in Hubble Space Telescope images of the northern and southern Jovian hemispheres obtained in [2000][2001][2002][2003][2004][2005][2006][2007]. On average, one feature is observed every day, but several auroral structures are occasionally seen over a wide range of local times in the same image. Several properties of these features are analyzed, such as their location, emitted power, and lifetime. Additionally, we magnetically map the auroral features to the equatorial plane using the VIPAL model in order to compare their observed properties with those of magnetospheric injections detected by the Galileo spacecraft. The equatorward auroral features show up between the Io footpath and the main auroral emission, at all System III longitudes, in agreement with Galileo measurements. Moreover, we compare the magnetic flux associated with these features with estimates of the outgoing flux related to the radial transport of plasma in the Jovian magnetosphere, and we find that they could account for at least one third of this flux. This comparative study shows that the auroral features under study are most probably related to magnetospheric injections and thus sheds light on the processes involved in the magnetosphere-ionosphere dynamics.

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Section: Introductionmentioning

confidence: 60%

Jupiter's equatorward auroral features: Possible signatures of magnetospheric injections

et al. 2014

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“…This is considerably larger than the CML ~ 150°–210° range where the northern aurora is most easily viewed [e.g., Connerney et al , ; Nichols et al , ], so that this phenomenon is not likely an artifact of auroral visibility. The first three brightening events were uncorrelated with solar wind variations (although it may be noteworthy that they occurred when the solar wind ram pressure was less than 0.1 nPa) and may be connected with the sudden release of plasma down Jupiter's magnetotail, as might be expected to occur during rotationally driven reconnection [e.g., Cowley et al , ; Kronberg et al , ; Louarn et al , ; Delamere et al , ; Walker and Jia , ], since they appear to have similar occurrence rates (every 2–4 days, when active). The time evolution of these three events is similar and is fairly well represented by exponentials with a 1/ e risetime of ~2 h and a 1/ e decay time of ~5 h. These events appear to be similar in all respects to those seen earlier with the Hisaki spacecraft [ Kimura et al , ].…”

Section: Resultsmentioning

confidence: 99%

Juno‐UVS approach observations of Jupiter's auroras

Gladstone

Versteeg

Greathouse

et al. 2017

Geophysical Research Letters

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Juno ultraviolet spectrograph (UVS) observations of Jupiter's aurora obtained during approach are presented. Prior to the bow shock crossing on 24 June 2016, the Juno approach provided a rare opportunity to correlate local solar wind conditions with Jovian auroral emissions. Some of Jupiter's auroral emissions are expected to be controlled or modified by local solar wind conditions. Here we compare synoptic Juno‐UVS observations of Jupiter's auroral emissions, acquired during 3–29 June 2016, with in situ solar wind observations, and related Jupiter observations from Earth. Four large auroral brightening events are evident in the synoptic data, in which the total emitted auroral power increases by a factor of 3–4 for a few hours. Only one of these brightening events correlates well with large transient increases in solar wind ram pressure. The brightening events which are not associated with the solar wind generally have a risetime of ~2 h and a decay time of ~5 h.

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“…Plasmoids observed at Uranus, Jupiter, and Saturn have a similar loop‐like topology, which is indicative of internal driving (Jackman et al, ; Vogt et al, ). Mass loss in the internally driven magnetospheres of Jupiter and Saturn are dominated by diffusive‐based processes (e.g., Delamere et al, ; Kane et al, ; Kivelson & Southwood, ; Louarn et al, ), with plasmoid‐based loss contributing to only ~5–15% of the total production rate when applying the same analytical methods as presented above (Jackman et al, ; Vogt et al, ). Because the conservative lower limit of the mass‐loss calculation derived here is greater than corresponding estimates for Jupiter and Saturn, it is possible that plasmoid ejection may be a dominant mass‐loss mechanism at Uranus.…”

Section: Discussionmentioning

confidence: 99%

Voyager 2 constraints on plasmoid‐based transport at Uranus

DiBraccio

Gershman

2019

Geophysical Research Letters

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A magnetosphere controls a planet's evolution by suppressing or enhancing atmospheric loss to space. In situ measurements of Uranus' magnetosphere from the Voyager 2 flyby in 1986 provide the only direct evidence of magnetospheric transport processes responsible for this atmospheric escape at Uranus. Analysis of high‐resolution Voyager 2 magnetic field data in Uranus' magnetotail reveals the presence of a loop‐like plasmoid filled with planetary plasma traveling away from the planet. This first plasmoid observation in an Ice Giant magnetosphere elucidates that (1) both internal and external forces play a role in Uranus' magnetospheric dynamics, (2) magnetic reconnection contributes to the circulation of plasma and magnetic flux at Uranus, and (3) plasmoids may be a dominant transport mechanism for mass loss through Uranus' magnetotail.

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Magnetic Reconnection and Associated Transient Phenomena Within the Magnetospheres of Jupiter and Saturn

Cited by 12 publications

References 145 publications

Jupiter's equatorward auroral features: Possible signatures of magnetospheric injections

Jupiter's equatorward auroral features: Possible signatures of magnetospheric injections

Juno‐UVS approach observations of Jupiter's auroras

Voyager 2 constraints on plasmoid‐based transport at Uranus

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